Hostname: page-component-586b7cd67f-rdxmf Total loading time: 0 Render date: 2024-11-29T15:29:07.421Z Has data issue: false hasContentIssue false
  • English
  • Français

Improved Analysis of COMPTEL Solar Neutron Data, with Application to the 15 June 1991 Flare

Published online by Cambridge University Press:  13 May 2016

M. P. Toner ,
J. M. Ryan ,
A. L. MacKinnon ,
D. Bhattacharya ,
K. P. Macpherson ,
M. L. McConnell ,
G. Rank ,
A M Thompson  and
T. O'Neill
M. P. Toner
Affiliation:
Department of Physics and Astronomy, University of Glasgow, UK
J. M. Ryan
Affiliation:
Space Science Center, University of New Hampshire, USA
A. L. MacKinnon
Affiliation:
Department of Physics and Astronomy, University of Glasgow, UK
D. Bhattacharya
Affiliation:
Institute of Geophysics and Planetary Physics, University of California, Riverside, USA
K. P. Macpherson
Affiliation:
Centre for Astrophysics, University of Central Lancashire, UK
M. L. McConnell
Affiliation:
Space Science Center, University of New Hampshire, USA
G. Rank
Affiliation:
Max Planck Institut fr Extraterrestriche Physik, Germany
A M Thompson
Affiliation:
Department of Physics and Astronomy, University of Glasgow, UK now at Schlumberger Geoquest, Abingdon
T. O'Neill
Affiliation:
Institute of Geophysics and Planetary Physics, University of California, Riverside, USA

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Direct solar flare neutrons are a valuable diagnostic of high-energy ion acceleration in these events, and COMPTEL improves over all previous cosmic neutron detectors in its capacity for neutron energy measurement. Previous studies of COMPTEL neutron data have worked with an incomplete model of the instrumental response, applying energy-by-energy detection efficiencies. Here we employ statistical regularisation techniques with the full (Monte Carlo simulation derived) response matrix to produce improved estimates of neutron numbers and energy distribution. These techniques are applied to data from the well-observed 15 June 1991 flare. Our improved treatment of the instrumental response results in a reduction of 73% in total neutron numbers, compared with previously deduced values. Implications for the picture of primary ion acceleration in this flare are briefly discussed.

Type
Session VI: The Solar Wind and Heliosphere
Information
Symposium - International Astronomical Union , Volume 203: Recent Insights into the Physics of the Sun and Heliosphere: Highlights from Soho and Other Space Missions , 2001 , pp. 573 - 576
Copyright
Copyright © Astronomical Society of the Pacific 2001 

References

Chupp, E.L., et al., 1982, ApJ., 263, L95.CrossRefGoogle Scholar
Craig, I. J. D., Brown, J. C., 1986, Inverse Problems in Astronomy, Adam Hilger.Google Scholar
Kocharov, G. E., Chuikin, E. I., Kovaltsov, G. A., Usoskin, I. G., Kocharov, L. E., 1994, in High Energy Solar Phenomena - A New Era of Spacecraft Measurements, eds. Ryan, J M and Vestrand, W T, AIP.Google Scholar
Kocharov, L., et al., 1998, A&A 340, 257.Google Scholar
O'Neill, T., et al, 1993, Compton Symposium, St. Louis, AIP Conf. Proc., 280, 1112.Google Scholar
McConnell, M., 1994, in High Energy Solar Phenomena - A New Era of Spacecraft Measurements, eds. Ryan, J M and Vestrand, W T, AIP.Google Scholar
O'Neill, T., et al. 1994, 2nd Compton Symposium, Maryland, AIP Conf. Proc., 304, 536.Google Scholar
Rank, G., 1995, , Max Planck Institut.Google Scholar
Thompson, A. M., 1992, GUIPS Manual, University of Glasgow.Google Scholar
Thompson, A. M., Craig, I. J. D., 1992, A&A, 262, 359.Google Scholar